飑线的研究进展

飑线是一种线状的中尺度对流系统,发生时破坏力大,可以产生严重的经济损失和人员伤亡。在我国,几乎每年都会出现由飑线引起的巨大损失。近年来,国内外对飑线的研究不断发展,无论是从大尺度环流背景、形成机制、组织形式、内部结构还是维持机制都有了较为深入的研究。深入研究飑线的形成过程,对于预报和灾害预警、防护,都具有很重要的意义。     

Combining optical spectroscopy and interferometry

Modern optical spectrographs and optical interferometers push the limits in the spectral and spatial regime, providing important new tools for the exploration of the Universe. In this contribution I outline the complementary nature of spectroscopic and interferometric observations and discuss different strategies for combining such data. Most remarkable, the latest generation of “spectro‐interferometric” instruments combine the milliarcsecond angular resolution achievable with interferometry with spectral capabilities, enabling direct constraints on the distribution, density, kinematics, and ionization structure of the gas component in protoplanetary disks. I will present some selected studies from the field of star‐ and planet formation and hot star research in order to illustrate these fundamentally new observational opportunities. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Studies of accretion flows around rotating black holes – I. Particle dynamics in a pseudo-Kerr potential

We study the formation of the absorption features, called the cyclotron–annihilation lines, in the γ-spectra of the neutron stars (pulsars), owing to the fundamental quantum-electrodynamic effect of the one–photon pair creation in magnetized vacuum. As a result, we substantiate a new method for the determination of the neutron star magnetic fields B based on measuring the interval between the main annihilation and the first cyclotron–annihilation absorption lines. It is found that these lines may be easily resolved, and, consequently, the method is surely applicable if the following conditions are satisfied. (i) A γ-source has to be compact enough and located near a star, but not close to its magnetic poles. For instance, it may be a disc in the plane of a star magnetic equator with latitudinal angular width less than     and radial extent up to 25 per cent of the star radius. (ii) The source is to produce detectable γ-radiation at large angles ≳60° to the local magnetic field. Being situated in a closed field line region and having a broad radiation pattern, such a source is not what is usually considered in the context of the polar cap and outer gap models of the pulsar γ-emission dealing with open field lines only. (iii) Magnetic field strength must lie in a certain narrow interval with the centre at  ∼(3–4) × 10¹²  G. Its width depends on the star orientation and disc radial extend and in the most favourable case is about 20–30 per cent of its lower boundary. Finally, the influence of the star rotation on this method employment is considered and new possibilities arising from forthcoming polarization observations are briefly discussed.     

关于高维代数族的nef-值态射的结构

设M是有末端奇点的n维正规代数簇，L是M上的丰富线丛,（M,L）的数字有效值为τ=u/v（u、v是互素的正整数），φ：M→X是由（M，L）决定的nef-值态射，F是φ的一般纤维。通过研究τ的取值情况对（M，L）进行分类．给出了当u=n＋1，n时（M,L）和（F，LF）的较完整的分类，推广了一些文献的结果。     

Cosmological Constant, Minimal Mass and Electroweak Interaction

A lower bound for the mass of a rotating body is derived in the general relativity theory with positive cosmological term Λ. The bound suggests a neutrino rest mass ∼1 meV and a neutrino magnetic moment of 10⁻⁴¹ erg/gauss ∼ Planck's magnetic moment. A connection between gravity and electroweak interaction is suggested.     

关于高维代数族的nef-值态射的结构

设M是有末端奇点的n维正规代数簇,L是M上的丰富线丛,(M,L)的数字有效值为τ=uv(u、v是互素的正整数),:M→X是由(M,L)决定的nef-值态射,F是的一般纤维。通过研究τ的取值情况对(M,L)进行分类,给出了当u=n+1,n时(M,L)和(F,LF)的较完整的分类,推广了一些文献的结果。